We explore the production of WIMP annihilation \(\gamma \) -rays obtained with our secluded DM model by following the analysis given in Refs. [1]}, [2]}.
In Ref. [2]} it is concluded that the observed \(\gamma \) -ray spectrum is best fit by WIMPS with a mass \(\sim \)  20 – 50 GeV that annihilate to quarks with a cross section \(<\sigma _{ann} v> \ = {\cal {O}}(10^{-26})\)  cm\(^3\) s\(^{-1}\) . Motivated by that work, we consider here two specific cases for our seculded WIMP models, viz., WIMPS with masses of 20 GeV and 32 GeV. With the parameter choices for these models as given and discussed in Section , our results are compatible with the observed DM density as parametrized by the value \(\Omega h^2 \simeq 0.119\) , and also with the value for \(\langle \sigma _{ann} v\rangle \)  required to explain the proposed \(\gamma \) -ray excess from DM annihilation. We now proceed to demonstrate this more explicitly for the two WIMP mass models that we consider.
